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On the differential rotation of massive main-sequence stars

Lookup NU author(s): Professor Tamara Rogers

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Abstract

To date, asteroseismology has provided core-to-surface differential rotation measurements in eight main-sequence stars. These stars, ranging in mass from similar to 1.5-9M(circle dot), show rotation profiles ranging from uniform to counter-rotation. Although they have a variety of masses, these stars all have convective cores and overlying radiative regions, conducive to angular momentum transport by internal gravity waves (IGWs). Using two-dimensional numerical simulations, we show that angular momentum transport by IGWs can explain all of these rotation profiles. We further predict that, should high mass, faster rotating stars be observed, the core-to-envelope differential rotation will be positive, but less than one.

Publication metadata

Author(s): Rogers TM

Publication type: Article

Publication status: Published

Journal: The Astrophysical Journal. Letters

Year: 2015

Volume: 815

Issue: 2

Print publication date: 18/12/2015

Online publication date: 18/12/2015

Acceptance date: 10/11/2015

ISSN (print): 2041-8205

ISSN (electronic): 2041-8213

Publisher: Institute of Physics Publishing

URL: http://dx.doi.org/10.1088/2041-8205/815/2/L30

DOI: 10.1088/2041-8205/815/2/L30

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